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Non-Radial Oscillations

Published online by Cambridge University Press:  07 February 2017

P. Ledoux*
Affiliation:
Institut d'Astrophysique, Université de Liège, Belgium

Abstract

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The problem of the adiabatic non-radial oscillations of spherical stars is reviewed and results recalled for a variety of models. The anomalous behaviour of the eigenfunctions for highly condensed models is related to the apparent mobile singularities depending on the eigenvalues. Tables of Q-values are provided to facilitate possible applications to variable stars.

In the case of the gravity modes, the existence of multiple spectra some stable (g+ modes) some unstable (g modes) if superadiabatic and subadiabatic regions alternate is discussed and the interest of further investigations underlined.

As far as vibrational stability (effects of the non adiabatic terms) is concerned, a general expression is given for the ‘damping coefficient’. The attention is drawn to the possibility for g+ modes of becoming vibrationally unstable under the effect of various factors and in various models, including the Sun where this was advocated as a possibility of relieving the neutrinos difficulty.

Finally the present status of the most obvious candidates among variable stars for non-radial oscillations, the β Canis Majoris stars and the rapid blue variables (white dwarfs) is briefly reviewed.

Type
Part VI Instability Mechanisms
Copyright
Copyright © Reidel 1974 

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